The figure below shows a summary of the process of low mass star formation as we believe it may proceed in massive star environments:

Low mass star formation in massive star environments is strongly affected by the presence of the massive stars themselves. Building on ideas originally published by Hester et al. (1996), we propose a specific and predictive scenario for low mass star formation in these environments. In our scenario, low mass star formation is originally triggered by the shock driven into molecular material by the advance of the photoionization front. Star forming cores are then overrun by the advancing ionization front within a few $10^5$ years. As these cores emerge into the H~II region interior, they go through a short-lived phase during which the dense core itself photoevaporates. This EGG phase, seen in M16 and other regions, lasts for a few $10^4$ years. When the core has evaporated, the circumstellar disk is itself exposed to UV from the massive stars, and so the object transitions into an "evaporating disk" phase, such as that seen in Orion. But this phase is also short lived. Within a few $10^4$ years, photoevaporation has eaten away the gaseous disk down to within a few tens of AU of the central YSO. This object then lives within the ionized, low density interior of the H~II region for the remainder of the lifetime of the region, which continues until the massive stars go supernovae. When those supernovae occur, the disks surrounding nearly low mass YSOs are pelted with ejecta from those supernovae. It is this process which ejects recently synthesized short-lived radionuclides into those disks.