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We set out to compare the age-metallicity relation (AMR) of massive clustersfrom Magellanic Cloud mass galaxies in the E-MOSAICS suite of numericalcosmological simulations with an amalgamation of observational data of massiveclusters in the Large and Small Magellanic Clouds (LMC/SMC). We aim to test if:i) star cluster formation proceeds according to universal physical processes,suggestive of a common formation mechanism for young-massive clusters (YMCs),intermediate-age clusters (IACs), and ancient globular clusters (GCs); ii)massive clusters of all ages trace a continuous AMR; iii) the AMRs of smallermass galaxies show a shallower relation when compared to more massive galaxies.Our results show that, within the uncertainties, the predicted AMRs ofL/SMC-mass galaxies with similar star formation histories to the L/SMC followthe same relation as observations. We also find that the metallicity at whichthe AMR saturates increases with galaxy mass, which is also found for the fieldstar AMRs. This suggests that relatively low-metallicity clusters can stillform in dwarfs galaxies. Given our results, we suggest that ancient GCs sharetheir formation mechanism with IACs and YMCs, in which GCs are the result of auniversal process of star cluster formation during the early episodes of starformation in their host galaxies.

Linking globular cluster formation at low and high redshift through the age-metallicity relation in E-MOSAICS