We carried out a pebble-driven planet formation simulations to investigate the formation of giant planets around intermediate-mass stars, in the stellar mass range between 1.5 M? and 3 M? [3]. We find that the massive giant planets are preferred to emerge in the circumstances when the disks have larger sizes, metallicities, and/or higher disk accretion rates. As these properties are only enhanced with stellar mass, an alternative physical scenario is needed to explain the decline of giant planet frequency from 2 to 3 M?. We propose that FUV/EUV photoevaporation in this stellar mass range plays a role in actively removing the disc, and slowing down planet formation. This photoevaporation mechanism is only dominant after the first 2Myr, meaning that, in this scenario, giant planets form predominantly later than the first couple of Myr of disc evolution. This is not in contradiction with the ~2Myr disc lifetimes found observationally, because only a small fraction of stars (long-lived discs) end up becoming giant planet hosts.