Star clusters form within molecular gas regions of high density, which are formed either upon the collapse of cold gas clouds or due to turbulent forces acting on the gas. We focus on star formation that takes place in the center of a spherically symmetric molecular gas cloud, which collapses under its own gravity. We investigate the conditions when the stellar feedback can slow down the collapse or even disrupt the cloud, potentially explaining the observed star formation efficiency in GMCs by means of self disruption of the cloud. When the gravitational force is dominant, secondary star-forming, continuous or monolithic, events are expected to occur. We built an one-dimensional model that is based on the hydrodynamic code FLASH and implements the fundamental physics of the feedback: ram pressure from the stellar winds, radiation pressure on dust and gas, and photoionization. We employ our model to discuss the probability that the compact cluster R136 in the Large Magellanic Cloud was formed due to feedback processes between NGC2070 and the massive cloud host. As clouds with constant density appear to collapse with high efficiency, we suggest a model of a cloud with centrally concentrated gas as essential for generating a self-disrupting feedback. This value of critical star formation efficiency is shown to be highly dependent on the cloud compactness.