An exhaustive chemical characterization of dense cores is mandatory to our understanding of chemical composition changes from a starless to a protostellar stage. However, only a few sources have had their molecular composition characterized in detail. Here we present a 3mm line survey of L483, a dense core around a Class 0 protostar, which was observed with the IRAM 30m telescope in the 80-116GHz frequency range. We detected 71 molecules (140 including different isotopologs), most of which are present in the cold and quiescent ambient cloud according to their narrow lines (FWHM~0.5km/s) and low rotational temperatures (<~10K). Of particular interest among the detected molecules are the cis isomer of HCOOH, the complex organic molecules HCOOCH_3_, CH_3_OCH_3_, and C_2_H_5_OH, a wide variety of carbon chains, nitrogen oxides like N_2_O, and saturated molecules like CH_3_SH, in addition to eight new interstellar molecules (HCCO, HCS, HSC, NCCNH^+^, CNCN, NCO, H_2_NCO^+^, and NS^+^) whose detection has already been reported. In general, fractional molecular abundances in L483 are systematically lower than in TMC-1 (especially for carbon chains), tend to be higher than in L1544 and B1-b, and are similar to those in L1527. Apart from the overabundance of carbon chains in TMC-1, we find that L483 does not have a marked chemical differentiation with respect to starless/prestellar cores like TMC-1 and L1544, although it does chemically differentiate from Class 0 hot corino sources like IRAS 16293-2422. This fact suggests that the chemical composition of the ambient cloud of some Class 0 sources could be largely inherited from the dark cloud starless/prestellar phase. We explore the use of potential chemical evolutionary indicators, such as the HNCO/C_3_S, SO_2_/C_2_S, and CH_3_SH/C_2_S ratios, to trace the prestellar/protostellar transition. We also derived isotopic ratios for a variety of molecules, many of which show isotopic ratios close to the values for the local interstellar medium (remarkably all those involving ^34^S and ^33^S), while there are also several isotopic anomalies like an extreme depletion in ^13^C for one of the two isotopologs of c-C_3_H_2_, a drastic enrichment in ^18^O for SO and HNCO (SO being also largely enriched in ^17^O), and different abundances for the two ^13^C substituted species of C_2_H and the two ^15^N substituted species of N_2_H^+^. We report the first detection in space of some minor isotopologs and quantify for the first time the deuterium fractionation for HDCCO and c-C_3_D. The exhaustive chemical characterization of L483 presented here, together with similar studies of other prestellar and protostellar sources, should allow us to identify the main factors that regulate the chemical composition of cores along the process of formation of low-mass protostars.