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We present the analysis of the properties of large samples of protostellardiscs formed in four radiation hydrodynamical simulations of star clusterformation. The four calculations have metallicities of 0.01, 0.1, 1 and 3 timessolar metallicity. The calculations treat dust and gas temperatures separatelyand include a thermochemical model of the diffuse interstellar medium. We findthe radii of discs of bound protostellar systems tend to decrease withdecreasing metallicity, with the median characteristic radius of discs in the0.01 and 3 times solar metallicity calculations being $\approx20$ and$\approx65$ au, respectively. Disc masses and radii of isolated protostars alsotend to decrease with decreasing metallicity. We find that the circumstellardiscs and orbits of bound protostellar pairs, and the two spins of the twoprotostars are all less well aligned with each other with lower metallicitythan with higher metallicity. These variations with metallicity are due toincreased small scale fragmentation due to lower opacities and greater coolingrates with lower metallicity, which increase the stellar multiplicity andincrease dynamical interactions. We compare the disc masses and radii ofprotostellar systems from the solar metallicity calculation with recent surveysof discs around Class 0 and I objects in the Orion and Perseus star-formingregions. The masses and radii of the simulated discs have similar distributionsto the observed Class 0 and I discs.

The statistical properties of protostellar discs and their dependence on metallicity