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We have run direct N-body simulations to investigate the impact of stellarevolution and dynamics on the structural properties of young massive (3x10^4solar masses) star clusters (SCs) with different metallicities (Z=1, 0.1, 0.01solar metallicity). Metallicity drives the mass loss by stellar winds andsupernovae (SNe), with SCs losing more mass at high metallicity. We havesimulated three sets of initial conditions, with different initial relaxationtimescale. We find that the evolution of the half-mass radius of SCs depends onhow fast two-body relaxation is with respect to the lifetime of massive stars.If core collapse is slow in comparison with stellar evolution, then mass lossby stellar winds and SNe is the dominant mechanism driving SC evolution, andmetal-rich SCs expand more than metal-poor ones. In contrast, if core collapseoccurs on a comparable timescale with respect to the lifetime of massive stars,then SC evolution depends on the interplay between mass loss and three-bodyencounters: dynamical heating by three-body encounters (mass loss by stellarwinds and SNe) is the dominant process driving the expansion of the core inmetal-poor (metal-rich) SCs. As a consequence, the half-mass radius ofmetal-poor SCs expands more than that of metal-rich ones. We also find coreradius oscillations, which grow in number and amplitude as metallicitydecreases.

The impact of metallicity-dependent mass loss versus dynamical heating on the early evolution of star clusters