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(abridged) A scenario for the formation of multiple co-eval populationsseparated in age by about 1 Myr in very young clusters (VYCs, ages less than 10Myr) and with masses in the range 600-20000 Msun is outlined. It rests upon aconverging inflow of molecular gas building up a first population of pre-mainsequence stars. The associated just-formed O stars ionise the inflow andsuppress star formation in the embedded cluster. However, they typically ejecteach other out of the embedded cluster within 10^6 yr, that is before themolecular cloud filament can be ionised entirely. The inflow of molecular gascan then resume forming a second population. This sequence of events can berepeated multiply. This model is applied to the Orion Nebula Cluster (ONC), inwhich three well-separated pre-main sequences in the color-magnitude diagram ofthe cluster have recently been discovered. The mass-inflow history isconstrained using this model and the number of OB stars ejected from eachpopulation are estimated for verification using Gaia data. As a consequence ofthe proposed model, the three runaway O star systems, AE Aur, mu Col and iotaOri, are considered as significant observational evidence for stellar-dynamicalejections of massive stars from the oldest population in the ONC.

Evidence for feedback and stellar-dynamically regulated bursty star cluster formation: the case of the Orion Nebula Cluster