  We present a theoretical investigation of multifilter (U,B,V, I and K) light
and radial velocity curves of five Classical Cepheids in NGC 1866, a young
massive cluster of the Large Magellanic Cloud. The best fit models accounting
for the luminosity and radial velocity variations of the five selected
variables, four pulsating in the fundamental mode and one in the first
overtone, provide direct estimates of their intrinsic stellar parameters and
individual distances. The resulting stellar properties indicate a slightly
brighter Mass Luminosity relation than the canonical one, possibly due to mild
overshooting and/or mass loss. As for the inferred distances, the individual
values are consistent within the uncertainties. Moreover, their weighted mean
value corresponds to a distance modulus of 18.56 + - 0.03 (stat) + - 0.1 (syst)
mag, in agreement with several independent results in the literature.
