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We investigate radiative feedback from a 34 M$_\odot$ star in a $10^4$M$_\odot$ turbulent cloud using three-dimensional radiation-hydrodynamics (RHD)models. We use Monte Carlo radiative transfer to accurately computephotoionization equilibrium and radiation pressure, with multiple atomicspecies and silicate dust grains. We include the diffuse radiation field, dustabsorption/re-emission, and scattering. The cloud is efficiently dispersed,with 75 per cent of the mass leaving the (32.3 pc)$^3$ grid within 4.3 Myr (1.1$t_{ff}$). This compares to all mass exiting within 1.6 Myr (0.74 $t_{ff}$) inour previously published $10^3$ M$_\odot$ cloud. At most 20 per cent of themass is ionized, compared to 40 per cent in the lower mass model, despite theionized volume fraction being 80 per cent in both, implying the higher masscloud is more resilient to feedback. The total Jeans-unstable mass increaseslinearly up to 1500 M$_\odot$ before plateauing after 2 Myr, corresponding to acore formation efficiency of 15 per cent. We also measure the time-variation ofthe far-ultraviolet (FUV) radiation field, $G_0$, impinging on other clustermembers, taking into account for the first time how this changes in a dynamiccluster environment with intervening opacity sources and stellar motions. Manyobjects remain shielded in the first 0.5 Myr whilst the massive star isembedded, after which $G_0$ increases by orders of magnitude. Gas motions lateron cause comparable drops which happen instantaneously and last for $\sim$ 1Myr before being restored. This highly variable UV field will influence thephotoevaporation of protoplanetary discs near massive stars.

Massive star feedback in clusters: variation of the FUV interstellar radiation field in time and space