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B-type stars are known to rotate at various velocities, including very fastrotators near the critical velocity as the Be stars. In this paper, we providestellar models covering the mass range between 1.7 to 15 Msun, which includesthe typical mass of known Be stars, at Z = 0.014, 0.006, and 0.002 and for anextended range of initial velocities on the zero-age main sequence. We used theGeneva stellar-evolution code, including the effects of shellular rotation,with a numerical treatment that has been improved so the code can preciselytrack the variation in the angular momentum content of the star as it changesunder the influence of radiative winds and/or mechanical mass loss. We discussthe impact of the initial rotation rate on the tracks in theHertzsprung-Russell diagram, the main-sequence (MS) lifetimes, the evolution ofthe surface rotation and abundances, as well as on the ejected masses ofvarious isotopes. Among the new results obtained from the present grid we findthat 1) fast-rotating stars with initial masses around 1.7 Msun present at thebeginning of the core hydrogen-burning phase quite small convective cores withrespect to their slowly rotating counterparts. This fact may be interesting tokeep in mind in the framework of the asteroseismic studies of such stars. 2)The contrast between the core and surface angular velocity is higher in slowerrotating stars. The values presently obtained are in agreement with the veryfew values obtained for B-type stars from asteroseismology. 3) At Z = 0.002,the stars in the mass range of 1.7 to 3 Msun with a mean velocity on the MS ofthe order of 150 km/s show N/H enhancement superior to 0.2 dex at mid-MS, andsuperior to 0.4 dex at the end of the MS phase. At solar metallicity thecorresponding values are below 0.2 dex at any time in the MS.

Populations of rotating stars. - I. Models from 1.7 to 15 Msun at Z = 0.014, 0.006, and 0.002 with {\Omega}/{\Omega}crit between 0 and 1