  We performed a new and accurate fit of light and radial velocity curves of
the Large Magellanic Cloud (LMC) Cepheid --OGLE-LMC-CEP-0227-- belonging to a
detached double-lined eclipsing binary system. We computed several sets of
nonlinear, convective models covering a broad range in stellar mass, effective
temperature and in chemical composition. The comparison between theory and
observations indicates that current theoretical framework accounts for
luminosity --V and I band-- and radial velocity variations over the entire
pulsation cycle. Predicted pulsation mass --M=4.14+-0.06 Mo-- and mean
effective temperature --Te=6100+-50 K-- do agree with observed estimates with
an accuracy better than 1 sigma. The same outcome applies, on average, to the
luminosity amplitudes and to the mean radius. We find that the best fit
solution requires a chemical composition that is more metal--poor than typical
LMC Cepheids (Z=0.004 vs 0.008) and slightly helium enhanced (Y=0.27 vs 0.25),
but the sensitivity to He abundance is quite limited. Finally, the best fit
model reddening --E(V-I)=0.171+-0.015 mag-- and the true distance modulus
corrected for the barycenter of the LMC --mu_{0,LMC}=18.50+-0.02+-0.10 (syst)
mag--, agree quite well with similar estimates in the recent literature.
