  The evolution of circumstellar discs is highly influenced by their
surroundings, in particular by external photoevaporation due to nearby stars
and dynamical truncations. The impact of these processes on disc populations
depends on the dynamical evolution of the star-forming region. Here we
implement a simple model of molecular cloud collapse and star formation to
obtain primordial positions and velocities of young stars and follow their
evolution in time, including that of their circumstellar discs. Our disc model
takes into account viscous evolution, internal and external photoevaporation,
dust evolution, and dynamical truncations. The disc evolution is resolved
simultaneously with the star cluster dynamics and stellar evolution. Our
results show that an extended period of star formation allows for massive discs
formed later in the simulations to survive for several million years. This
could explain massive discs surviving in regions of high UV radiation.
