Most stars form in the gravitational collapse of giant molecular clouds, where several stars are born from the same cloud in a single event. Observationally, gravitationally bound stellar clusters are the long lasting remnants of this formation. However, the initial cloud conditions, and physical processes which cause stars to remain gravitationally bound remain highly uncertain, causing a disconnect between the best star formation models and the observational remnants. In this work, we seek to bridge this gap by examining the 3D radiative magnetohydrodynamical STARFORGE simulations, which fully account for both stellar feedback, and gravitational evolution with extremely high resolution. In this simulation suite, we investigate the necessary conditions which result in a gravitationally bound cluster, and how viewing angle affects our ability to observationally determine what is a ‘cluster’. We also examine the embedded stage of cluster formation, describing timescales stars emerge from their natal clouds, and what is observable during these periods.
