  The main scope of this paper is to investigate the possible existence of a
metallicity dependence of the overshooting from main sequence stars turbulent
cores. We focus on objects with masses in the range ~2.5 Msol - ~25 Msol.
Basically, evolutionary time scale ratios are compared with star numbers ratios
on the main sequence. Star populations are synthesized using grids of
evolutionary tracks computed with various overshooting amounts. Observational
material is provided by the large and homogeneous photometric database of OGLE
2 project for the Magellanic clouds. Attention is paid to the study of
uncertainties: distance modulus, intergalactic and interstellar reddening, IMF
slope and average binarity rate. Rotation and chemical composition gradient are
also considered. The result for the overshooting distance is l_over(SMC)= 0.40
+0.12-0.06 Hp (Z=0.004) and l_over(LMC)= 0.10+0.17-0.10 Hp (Z=0.008) suggesting
a possible dependence of the extent of the mixed central regions with
metallicity within the considered mass range. Unfortunately it is not yet
possible to fully disentangle effects of mass and chemical composition.
