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Nuclear star clusters (NSCs) are the densest stellar systems in the Universeand are found in the centres of all types of galaxies. They are thought to formvia mergers of star clusters such as ancient globular clusters (GCs) thatspiral to the centre as a result of dynamical friction or through in-situ starformation directly at the galaxy centre. There is evidence that both pathsoccur, but the relative contribution of either channel and their correlationwith galaxy properties are not yet constrained observationally. We aim toderive the dominant NSC formation channel for a sample of 25 nucleatedgalaxies, mostly in the Fornax galaxy cluster, with stellar masses between$M_\rm{gal} \sim 10^8$ and $10^{10.5} M_\odot$ and NSC masses between$M_\rm{NSC} \sim 10^5$ and $10^{8.5} M_\odot$. Using Multi-Unit SpectroscopicExplorer (MUSE) data from the Fornax 3D survey and the ESO archive, we derivestar formation histories, mean ages and metallicities of NSCs, and compare themto the host galaxies. In many low-mass galaxies, the NSCs are significantlymore metal-poor than the hosts with properties similar to GCs. In contrast, inthe massive galaxies, we find diverse star formation histories and cases ofongoing or recent in-situ star formation. Massive NSCs ($> 10^7 M_\odot$)occupy a different region in the mass-metallicity diagram than lower mass NSCsand GCs, indicating a different enrichment history. We find a clear transitionof the dominant NSC formation channel with both galaxy and NSC mass. Wehypothesise that while GC-accretion forms the NSCs of the dwarf galaxies,central star formation is responsible for the efficient mass build up in themost massive NSCs in our sample. At intermediate masses, both channels cancontribute. The transition between these formation channels seems to occur atgalaxy masses $M_\rm{gal} \sim 10^9 M_\odot$ and NSC masses $M_\rm{NSC} \sim10^7 M_\odot$.

Diversity of nuclear star cluster formation mechanisms revealed by their star formation histories