Context : Aims : Many topical astrophysical research areas , such as the properties of planet host stars , the nature of the progenitors of different types of supernovae and gamma ray bursts , and the evolution of galaxies , require complete and homogeneous sets of stellar models at different metallicities in order to be studied during the whole of cosmic history . We present here a first set of models for solar metallicity , where the effects of rotation are accounted for in a homogeneous way . Methods : We computed a grid of 48 different stellar evolutionary tracks , both rotating and non-rotating , at Z = 0.014 , spanning a wide mass range from 0.8 to 120 M _ { \sun } . For each of the stellar masses considered , electronic tables provide data for 400 stages along the evolutionary track and at each stage , a set of 43 physical data are given . These grids thus provide an extensive and detailed data basis for comparisons with the observations . The rotating models start on the zero-age main sequence ( ZAMS ) with a rotation rate \upsilon _ { \text { ini } } / \upsilon _ { \text { crit } } = 0.4 . The evolution is computed until the end of the central carbon-burning phase , the early asymptotic giant branch ( AGB ) phase , or the core helium-flash for , respectively , the massive , intermediate , and both low and very low mass stars . The initial abundances are those deduced by Asplund and collaborators , which best fit the observed abundances of massive stars in the solar neighbourhood . We update both the opacities and nuclear reaction rates , and introduce new prescriptions for the mass-loss rates as stars approach the Eddington and/or the critical velocity . We account for both atomic diffusion and magnetic braking in our low-mass star models . Results : The present rotating models provide a good description of the average evolution of non-interacting stars . In particular , they reproduce the observed main-sequence width , the positions of the red giant and supergiant stars in the Hertzsprung-Russell ( HR ) diagram , the observed surface compositions and rotational velocities . Very interestingly , the enhancement of the mass loss during the red-supergiant stage , when the luminosity becomes supra-Eddington in some outer layers , help models above 15-20 M _ { \sun } to lose a significant part of their hydrogen envelope and evolve back into the blue part of the HR diagram . This result has interesting consequences for the blue to red supergiant ratio , the minimum mass for stars to become Wolf-Rayet stars , and the maximum initial mass of stars that explode as type II-P supernovae . Conclusions :