There has been increasing acknowledgement that most stars (and their protoplanetary discs) form in massive stellar clusters. The UV radiation field emitted by the massive stars in such clusters can affect protoplanetary discs via external photoevaporation, where UV radiation heats and disperses material from disc surfaces. Past planet formation and evolution models generally use either extended long-lived discs neglecting external photoevaporation or include some prescription of external photoevaporation that is tuned to produce disc lifetimes consistent with observations. However, realistically the interplay between the ongoing star formation and disc evolution/planet formation in a dynamically evolving cluster is much more complicated. Stars form at different times and locations in clusters, with some stars being initially embedded in star forming clouds that later disperse. It is almost unexplored how planet formation in discs around stars in such cluster environment is affected. Recently I performed the first calculations modelling disc evolution in a stellar cluster formation and feedback simulation model (Qiao et al. 2022). I will discuss the impacts of the time varying UV radiation and shielding of the clouds on disc evolution, and new work (Qiao et al. in prep.) in which we investigate the impacts on planet formation (and migration) via pebble accretion. We demonstrate that external photo-evaporation is effective in reducing the mass reservoir of solids that can be converted into pebbles and so hindering planet growth. We also demonstrate the importance of disc shielding time in preventing mass loss and radius truncation in early disc evolution, and therefore preserve the solid mass reservoir available for planet formation via pebble accretion.