  Seventy-two grids of stellar evolutionary tracks, along with the capability
to generate isochrones and luminosity/color functions from them, are presented
in this investigation. Sixty of them extend (and encompass) the sets of models
reported by VandenBerg et al. (2000, ApJ, 532, 430) for 17 [Fe/H] values from
-2.31 to -0.30 and alpha-element abundances corresponding to [alpha/Fe] = 0.0,
0.3, and 0.6 (at each iron abundance) to the solar metallicity and to
sufficiently high masses (up to ~2.2 solar masses) that isochrones may be
computed for ages as low as 1 Gyr. The remaining grids contain tracks for
masses from 0.4 to 4.0 solar masses and 12 [Fe/H] values between -0.60 and
+0.49 (assuming solar metal-to-hydrogen number abundance ratios): in this case,
isochrones may be calculated down to ~0.2 Gyr. The extent of convective core
overshooting has been modelled using a parameterized version of the Roxburgh
(1989, A&A, 211, 361) criterion, in which the value of the free parameter at a
given mass and its dependence on mass have been determined from analyses of
binary star data and observed color-magnitude diagrams for several open
clusters. Because the calculations reported herein satisfy many empirical
constraints, they should provide useful probes into the properties of both
simple and complex stellar populations. [All of the model grids may be obtained
from the Canadian Astronomy Data Center
(http://www.cadc-ccda.hia-iha.nrc-cnrc.gc.ca/cvo/community/VictoriaReginaModels
).]
