  B-type stars are known to rotate at various velocities, including very fast
rotators near the critical velocity as the Be stars. In this paper, we provide
stellar models covering the mass range between 1.7 to 15 Msun, which includes
the typical mass of known Be stars, at Z = 0.014, 0.006, and 0.002 and for an
extended range of initial velocities on the zero-age main sequence. We used the
Geneva stellar-evolution code, including the effects of shellular rotation,
with a numerical treatment that has been improved so the code can precisely
track the variation in the angular momentum content of the star as it changes
under the influence of radiative winds and/or mechanical mass loss. We discuss
the impact of the initial rotation rate on the tracks in the
Hertzsprung-Russell diagram, the main-sequence (MS) lifetimes, the evolution of
the surface rotation and abundances, as well as on the ejected masses of
various isotopes. Among the new results obtained from the present grid we find
that 1) fast-rotating stars with initial masses around 1.7 Msun present at the
beginning of the core hydrogen-burning phase quite small convective cores with
respect to their slowly rotating counterparts. This fact may be interesting to
keep 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 slower
rotating stars. The values presently obtained are in agreement with the very
few 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 of
the order of 150 km/s show N/H enhancement superior to 0.2 dex at mid-MS, and
superior to 0.4 dex at the end of the MS phase. At solar metallicity the
corresponding values are below 0.2 dex at any time in the MS.
