Abstract：Over the past decades, the discovery of a large number of young massive clusters (YMCs) in the local Universe and giant clumps in high-z galaxies suggests that clustered star formation is the dominant star formation mode. Mass and energy feedback from these enormous clusters is inevitably responsible for shaping the properties of their host galaxies. To model star formation in a more realistic way, I implemented a novel prescription in cosmological hydrodynamic simulations by treating star clusters as a unit of star formation. I tested this algorithm by running a suite of cosmological simulations with unprecedented parsec-scale spatial resolution. I found that various observed properties of host galaxies and star clusters are reproduced. Interestingly, we find some of these properties can be used to calibrate the subgrid models in the simulations. We follow the orbits of all simulated star clusters, estimate the cluster mass loss due to tidal disruption, and for the first time, investigate the connection between YMCs formed at high-z and the globular clusters observed at present. In parallel, to study how giant molecular clouds (GMCs) collapse to form star clusters and how they are eventually disrupted by stellar feedback from massive stars, I performed a suite of high-resolution hydrodynamic simulations of individual GMCs with self-consistent star formation and momentum feedback. I find that the final star cluster mass depends strongly on the surface density of the cloud due to the force balancing between gravity and momentum feedback.