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Ongoing studies with XMM–Newton have shown that powerful accretion disc winds, as revealed through highly ionized Fe K-shell absorption at E ≥ 6.7 keV, are present in a significant fraction of active galactic nuclei (AGNs) in the local Universe (Tombesi et al. ). In Gofford et al., we analysed a sample of 51 Suzaku-observed AGNs and independently detected Fe K absorption in ∼40 per cent of the sample, and we measured the properties of the absorbing gas. In this work, we build upon these results to consider the properties of the associated wind. On average, the fast winds (v_w > 0.01c) are located <r> ∼ 10¹⁵⁻¹⁸ cm (typically ∼10²⁻⁴ r_s) from their black hole, their mass outflow rates are of the order of $\langle \skew{3}\dot{M}_{\rm w}\rangle \sim 0.01\hbox{--}1$ M_⊙ yr⁻¹ or ${\sim }(0.01\hbox{--}1)\skew{3}\dot{M}_{\rm Edd}$ and kinetic power is constrained to <L_w> ∼ 10⁴³⁻⁴⁵ erg s⁻¹, equivalent to ∼(0.1–10 per …