In this work, we investigate if the location of galaxies within the large-scale structures (LSS) of the Universe leaves an imprint in their stellar mass (M*) and morphology. To this end, we attempt to disentangle the effects of local and large-scale environments in their distributions. We classify a sample of 25309 galaxies in the redshift range 0.02<z<=0.04 with log M*/M_{sun}_>=9.5 in terms of both the main LSS environments (voids, clusters, and not clusters nor voids, referred as NCNV) and local environment (singlets and multiplets; galaxies with and without companions). We present the stellar mass and morphology distributions in these environments, as well as for a subsample of galaxy pairs. Even in voids, we find that ~22% of galaxies have companions. Stellar mass distributions show that galaxies are significantly less massive in voids, regardless of their local environment. Satellites in voids are, too, less massive with respect to their centrals than in pairs of NCNV. In terms of morphology, the denser the LSS, the greater is the proportion of early-type galaxies, even among singlets. In voids and NCNV, late-type multiplets tend to be later-type spirals than singlets. In pairs, centrals tend to be more early-type than satellites. The sample, curated to avoid morphology incompleteness, results in slightly higher fractions of early-type galaxies and multiplets than previous studies. We conclude that local environment alone is not sufficient to explain the distribution of stellar mass and morphology of galaxies in the local Universe. The observed mass distributions are consistent with a scenario in which the assembly of galaxies depends critically on their host halos, and the properties of these halos are related to their large-scale environment. This would explain the finding of lower-mass galaxies in voids than in denser environments, and provide a basis for considering a common evolutionary origin for multiplets.