  Whether ionization feedback triggers the formation of massive stars is highly
debated. Using ALMA 3 mm observations with a spatial resolution of $\sim 0.05$
pc and a mass sensitivity of 1.1 $\rm M_\odot$ beam$^{-1}$ at 20 K, we
investigate the star formation and gas flow structures within the ionizing
feedback-driven structure, a clump-scale massive ($\gtrsim 1500$ $\rm M_\odot$)
bright-rimmed cloud (BRC) associated with IRAS 18290-0924. This BRC is bound
only if external compression from ionized gas is considered. A small-scale
($\lesssim1$ pc) age sequence along the direction of ionizing radiation is
revealed for the embedded cores and protostars, which suggests triggered star
formation via radiation-driven implosion (RDI). Furthermore, filamentary gas
structures converge towards the cores located in the BRC's center, indicating
that these filaments are fueling mass towards cores. The local core-scale mass
infall rate derived from H$^{13}$CO$^+$ $J=1-0$ blue profile is of the same
order of magnitude as the filamentary mass inflow rate, approximately 1 $\rm
M_\odot$ kyr$^{-1}$. A photodissociation region (PDR) covering the irradiated
clump surface is detected in several molecules, such as CCH, HCO$^+$, and CS
whereas the spatial distribution stratification of these molecules is
indistinct. CCH spectra of the PDR possibly indicate a photoevaporation flow
leaving the clump surface with a projected velocity of $\sim2$ km s$^{-1}$. Our
new observations show that RDI accompanied by a clump-fed process is operating
in this massive BRC. Whether this combined process works in other massive BRCs
is worth exploring with dedicated surveys.
