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We have computed stellar evolutionary models for stars in a mass rangecharacteristic of Cepheid variables ($3<m/\Msol<12$) for differentmetallicities representative of the Galaxy and the Magellanic Cloudspopulations. The stellar evolution calculations are coupled to a linear nonadiabatic stability analysis to get self-consistent mass-period-luminosityrelations. The period - luminosity relation as a function of metallicity isanalysed and compared to the recent EROS observations in the Magellanic Clouds.The models reproduce the observed width of the instability strips for the SMCand LMC. We determine a statistical P-L relationship, taking into account theevolutionary timescales and a mass distribution given by a Salpeter massfunction. Excellent agreement is found with the SMC PL relationship determinedby Sasselov et al. (1997). The models reproduce the change of slope in the P-Lrelationship near $P\sim 2.5$ days discovered recently by the EROScollaboration (Bauer 1997; Bauer et al. 1998) and thus explain this feature interm of stellar evolution. Some discrepancy, however, remains for the LMCCepheids. The models are also in good agreement with Beat Cepheids observed bythe MACHO and EROS collaborations. We show that most of the 1H/2H Beat Cepheidshave not yet ignited central helium burning; they are just evolving off theMain Sequence toward the red giant branch.Comment: 18 pages, Latex file, uses aasms4.sty, accepted for publication in  ApJ Letter

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