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We calculated a grid of evolutionary tracks of rotating models with massesbetween 1.0 and 3.0 $M_{\odot}$ and a resolution $\delta M \leq 0.02$$M_{\odot}$, which can be used to study the effects of rotation on stellarevolutions and on the characteristics of star clusters. The value of $\sim$2.05$M_{\odot}$ is a critical mass for the effects of rotation on stellar structureand evolution. For stars with $M >$ 2.05 $M_{\odot}$, rotation leads to anincrease in the convective core and prolongs the lifetime of main sequence(MS); rotating models evolve slower than non-rotating ones; the effects ofrotation on the evolution of these stars are similar to those of convectivecore overshooting. However for stars with 1.1 $< M/M_{\odot}<$ 2.05, rotationresults in a decrease in the convective core and shortens the lifetime of MS;rotating models evolve faster than non-rotating ones. When the mass is locatedin the range of $\sim$1.7 - 2.0 $M_{\odot}$, the mixing caused by rotationallyinduced instabilities is not efficient; the hydrostatic effects dominate theeffect on the evolution of these stars. For the models with masses betweenabout 1.6 and 2.0 $M_{\odot}$, rotating models always exhibit lower effectivetemperatures than non-rotating ones at the same age during the MS stage. For agiven age, the lower the mass, the smaller the change in the effectivetemperature. Thus rotations could lead to a color spread near the MS turnoff inthe color-magnitude diagram for the intermediate-age star clusters.

Grids of rotating stellar models with masses between 1.0 and 3.0 Msun