  Massive star clusters are observed in a broad range of galaxy luminosity and
types, and are assumed to form in dense gas-rich environments. Using a
parsec-resolution hydrodynamical simulation of an isolated gas-rich low mass
galaxy, we discuss here the non-linear effects of stellar feedback on the
properties of star clusters with a focus on the progenitors of nuclear
clusters. Our simulation shows two categories of star clusters: those for which
feedback expels gas leftovers associated with their formation sites, and those,
in a denser environment around which feedback fails at totally clearing the
gas. We confirm that radiation feedback (photo-ionization and radiative
pressure) plays a more important role than type-II supernovae in destroying
dense gas structures, and altering or quenching the subsequent cluster
formation. It also disturbs the cluster mass growth, by increasing the internal
energy of the gas component to the point when radiation pressure overcomes the
cluster gravity. We discuss how these effects may depend on the local
properties of the interstellar medium, and also on the details of the subgrid
recipes, which can affect the available cluster gas reservoirs, the evolution
of potential nuclear clusters progenitors, and the overall galaxy morphology.
