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Massive star clusters are ubiquitous in and around galaxies. The complex questions of their mass-size relation, chemical composition, star formation history, and even dark matter contents imply ties and yet differences with galaxy formation, which remain difficult to understand. In the Milky Way, massive clusters are confined to the halo, as old globular clusters. Indeed, our Galaxy is not forming massive clusters anymore, for an unknown reason. This means that the objects we can study with the best resolution and accuracy are also those the furthest from the physical conditions of their formation. But new instruments like JWST and Euclid are now pushing the limits further in the early Universe and extreme conditions, providing puzzling results on galaxy and star cluster formation. Simulations to the rescue! In this talk, I will present results from a collection of high resolution simulations of galaxies, isolated and in cosmological context, designed to propose new theoretical interpretations on the evolution of the physical conditions of star (cluster) forming galaxies. I will particularly illustrate the complex role of galaxy mergers and interactions in shaping (or not…) the interstellar medium and the star formation activity. This picture will be complemented with scenarios based on the sole intrinsic evolution of the galactic disks, without any external effects. I will conclude that the external and internal aspects conspire to drastically change the morphology, kinematics, and chemical history of Milky Way-like galaxies, and that these modifications imply the ending of the formation epoch for massive star clusters.
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