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Recent studies indicate that the progenitors of merging black hole (BH)binaries from young star clusters can undergo a common envelope phase just likeisolated binaries. If the stars emerge from the common envelope as naked cores,tidal interactions can efficiently synchronize their spins before they collapseinto BHs. Contrary to the isolated case, these binary BHs can also undergodynamical interactions with other BHs in the cluster before merging. Theinteractions can tilt the binary orbital plane, leading to spin-orbitmisalignment. We estimate the spin properties of merging binary BHs undergoingthis scenario by combining up-to-date binary population synthesis and accuratefew-body simulations. We show that post-common envelope binary BHs are likelyto undergo only a single encounter, due to the high binary recoil velocity andshort coalescence times. Adopting conservative limits on the binary-singleencounter rates, we obtain a local BH merger rate density of ~6.6 yr^-1 Gpc^-3.Assuming low (<0.2) natal BH spins, this scenario reproduces the trends in thedistributions of effective spin Xeff and precession parameters Xp inferred fromGWTC-2, including the peaks at (Xeff, Xp) ~ (0.1, 0.2) and the tail at negativeXeff values.

Spin misalignment of black hole binaries from young star clusters: implications for the origin of gravitational waves events