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The success of analytic waveform modeling within the effective-one-body (EOB)approach relies on the precise understanding of the physical importance of eachtechnical element included in the model. The urgency of constructingprogressively more sophisticated and complete waveform models (e.g. includingspin precession and eccentricity) partly defocused the research from a carefulcomprehension of each building block (e.g. Hamiltonian, radiation reaction,ringdown attachment). Here we go back to the spirit of the first EOB works. Wefocus first on nonspinning, quasi-circular, black hole binaries and analyzesystematically the mutual synergy between numerical relativity (NR) informedfunctions and the high post-Newtonian corrections (up to 5PN) to the EOBpotentials. Our main finding is that it is essential to correctly control thenoncircular part of the dynamics during the late plunge up to merger. We thenimprove the {\tt TEOBResumS-GIOTTO} waveform model for quasi-circular,spin-aligned black hole binaries. We obtain maximal EOB/NR unfaithfulness${\bar{F}}^{\rm max}_{\rm EOBNR}\sim 10^{-3}$ (with Advanced LIGO noise and inthe total mass range $10-200M_\odot$) for the dominant $\ell=m=2$ mode all overthe 534 spin-aligned configurations available through the Simulating eXtremeSpacetime catalog. The model performance, also including higher modes, is thenexplored using the NR surrogates \nrsurqeight{} and \nrsurqfifteen, to validateit up to mass ratio $m_1/m_2=15$. We find that, over the set of configurationsconsidered, more than $98\%$ of the total-mass-maximized unfaithfulness liebelow the $3\%$ threshold when comparing to the surrogate models.

Analytic systematics in next-generation of effective-one-body gravitational waveform models for future observations