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The star cluster initial mass function is observed to have an inverse powerlaw exponent around 2, yet there is no consensus on what determines thisdistribution, and why some variation is observed in different galaxies.Furthermore, the cluster formation efficiency covers a range of values,particularly when considering different environments. These clusters are oftenused to empirically constrain star formation and as fundamental units forstellar feedback models. Detailed galaxy models must therefore accuratelycapture the basic properties of observed clusters to be considered predictive.We use hydrodynamical simulations of a dwarf galaxy as a laboratory to studystar cluster formation. We test different combinations of stellar feedbackmechanisms, including stellar winds, ionizing radiation, and supernovae. Eachfeedback mechanism affects the cluster formation efficiency and cluster massfunction. Increasing the feedback budget by combining the different types offeedback decreases the cluster formation efficiency by reducing the number ofmassive clusters. Ionizing radiation is found to be especially influential.This effect depends on the timing of feedback initiation, as shown by comparingearly and late feedback. Early feedback occurs from ionizing radiation andstellar winds with onset immediately after a massive star is formed. Latefeedback occurs when energy injection only starts after the main-sequencelifetime of the most massive SN progenitor, a timing that is further influencedby the choice of the most massive SN progenitor. Late feedback alone results ina broad, flat mass function, approaching a log-normal shape in the completeabsence of feedback. Early feedback, on the other hand, produces a power-lawcluster mass function with lower formation efficiency, albeit with a steeperslope than that usually observed.

Pre-supernova feedback sets the star cluster mass function to a power law and reduces the cluster formation efficiency