  Victoria-Regina isochrones for $-0.4 \le$ [alpha/Fe] $\le +0.4$ and a wide
range in [Fe/H], along with complementary zero-age horizontal branch (ZAHB)
loci, have been applied to the color-magnitude diagram (CMD) of Carina. The
color transformations that we have used have been "calibrated" so that
isochrones provide excellent fits to the $[(B-V)_0,\,M_V]$-diagrams of M3 and
M92, when well supported estimates of the globular cluster (GC) reddenings and
metallicities are assumed. The adopted distance moduli, for both the GCs and
Carina, are based on our ZAHB models, which are able to reproduce the old HB
component (as well as the luminosity of the HB clump) of the dwarf spheroidal
galaxy quite well --- even if it spans a range in [Fe/H] of ~ 1.5 dex, provided
that [alpha/Fe] varies with [Fe/H] in approximately the way that has been
derived spectroscopically. Ages derived here agree reasonably well with those
found previously for the old and intermediate-age turnoff stars, as well as for
the period of negligible star formation (SF) activity (~ 6-10 Gyr ago). CMD
simulations have been carried out for the faintest turnoff and subgiant stars.
They indicate a clear preference for SF that lasted several Gyr instead of a
short burst, with some indication that ages decrease with increasing [Fe/H]. In
general, stellar models that assume spectroscopic metallicities provide
satisfactory fits to the observations, including the thin giant branch of
Carina, though higher oxygen abundances than those implied by the adopted
values of [alpha/Fe] would have favorable consequences.
