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The physics of star formation and the deposition of mass, momentum, andenergy into the interstellar medium by massive stars (`feedback') are the mainuncertainties in modern cosmological simulations of galaxy formation andevolution. These processes determine the properties of galaxies, but are poorlyunderstood on the $\lesssim$100 pc scale of individual giant molecular clouds(GMCs) resolved in modern galaxy formation simulations. The key question is whythe timescale for depleting molecular gas through star formation in galaxies($t_{\rm dep}\approx 2$ Gyr) exceeds the dynamical timescale of GMCs by twoorders of magnitude. Either most of a GMC's mass is converted into stars overmany dynamical times, or only a small fraction turns into stars before the GMCis dispersed on a dynamical timescale. Here we report our observation thatmolecular gas and star formation are spatially de-correlated on GMC scales inthe nearby flocculent spiral galaxy NGC300, contrary to their tight correlationon galactic scales. We demonstrate that this de-correlation implies rapidevolutionary cycling between GMCs, star formation, and feedback. We apply anovel statistical method to quantify the evolutionary timeline and find thatstar formation is regulated by efficient stellar feedback, driving GMCdispersal on short timescales (~1.5 Myr) due to radiation and stellar winds,prior to supernova explosions. This feedback limits GMC lifetimes to about onedynamical timescale (~10 Myr), with integrated star formation efficiencies ofonly 2-3%. Our findings reveal that galaxies consist of building blocksundergoing vigorous, feedback-driven lifecycles, that vary with the galacticenvironment and collectively define how galaxies form stars. Systematicapplications of this multi-scale analysis to large galaxy samples will providekey input for a predictive, bottom-up theory of galaxy formation and evolution.

Fast and inefficient star formation due to short-lived molecular clouds and rapid feedback