  The LMC clusters are unique templates of simple stellar population (SSP),
being crucial to calibrate models describing the integral light as well as to
test the stellar evolution theory. With this in mind we analyzed HST/WFPC2 (V,
B--V) colour-magnitude diagrams (CMDs) of 15 populous LMC clusters with ages
between ~0.3 Gyr and ~4 Gyr using different stellar evolutionary models
(Padova, PEL or Pisa, BaSTI or Teramo). Following the approach described by
Kerber, Santiago & Brocato (2007), we determined accurate and self-consistent
physical parameters (age, metallicity, distance modulus and reddening) for each
cluster by comparing the observed CMDs with synthetic ones. We found
significant trends in the physical parameters due to the choice of stellar
evolutionary model and treatment of convective core overshooting. In general,
models that incorporate overshooting presented more reliable results than those
that do not. Comparisons with the results found in the literature demonstrated
that our derived metallicities are in good agreement with the ones from the
spectroscopy of red giants. We also confirmed that, independent of the adopted
stellar evolutionary library, the recovered 3D distribution for these clusters
is consistent with a thick disk roughly aligned with the LMC disk as defined by
field stars. Finally, we also provide new estimates of distance modulus to the
LMC center, that are marginally consistent with the canonical value of 18.50.
