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We study star cluster formation in various environments with differentmetallicities and column densities by performing a suite of three-dimensionalradiation hydrodynamics simulations. We find that the photoionization feedbackfrom massive stars controls the star formation efficiency (SFE) in astar-forming cloud, and its impact sensitively depends on the gas metallicity$Z$ and initial cloud surface density $\Sigma$. At $Z=1~Z_{\odot}$, SFEincreases as a power law from 0.03 at $\Sigma = 10~M_{\odot}{\rm pc^{-2}}$ to0.3 at $\Sigma = 300~M_{\odot}{\rm pc^{-2}}$. In low-metallicity cases$10^{-2}- 10^{-1} Z_{\odot}$, star clusters form from atomic warm gases becausethe molecule formation time is not short enough with respect to the cooling ordynamical time. In addition, the whole cloud is disrupted more easily byexpanding H{\sc ii} bubbles which have higher temperature owing to lessefficient cooling. With smaller dust attenuation, the ionizing radiationfeedback from nearby massive stars is stronger and terminate star formation indense clumps. These effects result in inefficient star formation inlow-metallicity environments: the SFE drops by a factor of $\sim 3$ at$Z=10^{-2}~Z_{\odot}$ compared to the results for $Z=1~Z_{\odot}$, regardlessof $\Sigma$. Newborn star clusters are also gravitationally less bound. Wefurther develop a new semi-analytical model that can reproduce the simulationresults well, particularly the observed dependencies of the SFEs on the cloudsurface densities and metallicities.

Star cluster formation and cloud dispersal by radiative feedback: dependence on metallicity and compactness