The models are calculated for different chemical compositions both without overshooting (standard models, including microscopic diffusion of He and heavy elements) and with different overshooting efficiency. Each set of models can be found in a different sub-directory. It is possible to get all the content for each chemical composition, the content of each selected sub-directory or just a given file. In each directory there are evolutionary tracks (TRACKS), isochrones (ISOCHRONES), horizontal branch models together with a table of the ZAHB characteristics (HB) and files with some relevant physical values of selected models (STRUCTURES). Models with overshooting are calculated for masses higher than 1M_{sun}_ to avoid the unobserved presence of the overall contraction feature in 1M_{sun}_ stars. Thus isochrones for ages higher than about 5Gyr are the same as in the standard case and thus are not included in the overshooting directories. Models with overshooting does not include microscopic diffusion because for masses higher than about 1M_{sun}_ the effect of this mechanism is almost negligible. Models with overshooting are calculated for masses higher than 1M_{sun}_ to avoid the unobserved presence of the overall contraction feature in 1M_{sun}_ stars. Thus isochrones for ages higher than about 5Gyr are the same as in the standard case and thus are not included in the overshooting directories. Models with overshooting does not include microscopic diffusion because for masses higher than about 1M_{sun}_ the effect of this mechanism is almost negligible. All the tracks and isochrones have been transformed in the observation plane by adopting the model atmospheres by Castelli (1999A&A...346..564C), see also Castelli, Gratton & Kurucz (1997A&A...318..841C). For convenience, all tracks and isochrones have been grouped in 4 tables tracks.dat, struct.dat, hb.dat and isochron.dat