Protoclusters are dense regions of molecular gas that represent the earliest stages of stellar cluster formation and the birthplaces of massive stars. Understanding the physical processes that govern their evolution is therefore essential for building a complete picture of massive star formation. In this talk, I will present results from two recent ALMA-based studies that investigate the roles of turbulence, magnetic fields, and gravity in massive protocluster environments. First, I will discuss our analysis of the G327.29 protocluster, where dust polarization observations are compared with the Velocity Gradient Technique (VGT), which is based on the modern theory of magnetohydrodynamic turbulence, to infer magnetic field morphology in dense star-forming regions. This comparison provides new insight into the complex physical conditions of protocluster environments, where turbulence, magnetic fields, and gravity jointly shape the gas dynamics. I will then present results from our other work, where we investigate the properties of turbulence in fifteen massive protoclusters from the ALMA-IMF survey using the C¹⁸O spectral line. By analyzing the kinematic structure and turbulent velocity statistics across these regions, we find that turbulence is supersonic in nature and maintained throughout the evolutionary stages of massive protoclusters, likely sustained by feedback from expanding H II regions. Together, these results offer a broader view of how turbulence, magnetic fields, and gravity influence the structure and evolution of massive star-forming regions.