Abstract
The problem of the mass discrepancy of Cepheid stars in the young, rich LMC cluster NGC 2157, which is known to possess three Cepheids, is examined. The simultaneous fit of the color-magnitude diagram with theoretical simulations based on models for intermediate-mass stars incorporating either semiconvection or overshoot in the central cores, and with suited chemical composition, and tha derivation of the pulsational masses from the Cepheid models of Choisi & Wood allow us to show that the problem of mass discrepancy likely originates from the adoption of semiconvective models and insufficient accuracy in the determination of the mass by one of the two methods
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