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 \sim 2.5 \mathrm { M } _ { \sun } - \sim 25 \mathrm { M } _ { \sun } .
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 _ { \mathrm { over } } ^ { \mathrm { SMC } } = 0.40 ^ { +0.12 } _ { -0.06 } \mathrm { H } _ { \mathrm { p } } ( Z _ { 0 } = 0.004 ) and l _ { \mathrm { over } } ^ { \mathrm { LMC } } = 0.10 ^ { +0.17 } _ { -0.10 } \mathrm { H } _ { \mathrm { p } } ( Z _ { 0 } = 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 .