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Star clusters form in dense, hierarchically collapsing gas clouds. Bulkkinetic energy is transformed to turbulence with stars forming from cores fedby filaments. In the most compact regions, stellar feedback is least effectivein removing the gas and stars may form very efficiently. These are also theregions where, in high-mass clusters, ejecta from some kind of high-mass starsare effectively captured during the formation phase of some of the low massstars and effectively channeled into the latter to form multiple populations.Star formation epochs in star clusters are generally set by gas flows thatdetermine the abundance of gas in the cluster. We argue that there is likelyonly one star formation epoch after which clusters remain essentially clear ofgas by cluster winds. Collisional dynamics is important in this phase leadingto core collapse, expansion and eventual dispersion of every cluster. We reviewrecent developments in the field with a focus on theoretical work.

The Physics of Star Cluster Formation and Evolution