This thesis is focused on the role of stellar clusters of pre-main sequence (PMS)low-mass stars in the mechanisms leading to the formation of massive stars. We study the young low-mass stellar population in three nearby massive star-forming regions: Orion, DR21 and Monoceros R2. The characterization of this population is a challenge because it is usually still deeply embedded in the parental molecular cloud. Large amounts of dust and gas produce high extinctions that prevent their detection in the optical and even in the near-infrared (IR) wavelengths. Only X-ray,radio/(sub)millimeter and very deep IR observations are able to penetrate into the massive star cradles and reveal the low-mass stellar population. Thus, we use the X-ray catalogs provided by the space telescope Chandra, complementing them with deep IR surveys. We study the properties of the low-mass stellar population (such as the spatial distribution, the clustering, the stellar densities, the extinction distribution or the evolutionary phase) and discuss which massive star formation scenario better agrees with our results.Additionally, with the aim of better understanding both the properties of the members of these young clusters and the molecular environment of massive star cradles,we carry out new Very Large Array (VLA) radio continuum multi-epoch observations of Orion, and new Submillimeter Array (SMA) observations of the central region of Monoceros R2.To assess the impact of outflow feedback, we study the role of the outflow-driven turbulence in two clusters of outflows embedded in massive star-forming regions, such as the Orion OMC1-S region and the central region of Monoceros R2.