Initial parameter choices for all evolutions that reproduce Venus in a space defined by all of our varied parameters: the temperature jump across the core–mantle boundary (ΔT_CMB), the reference viscosity (ν_ref), the jump in viscosity from the upper to the lower mantle (ν_jump), the core liquidus depression (ΔT_χ,ref), the amount of potassium-40 in the mantle (⁴⁰K_man), the amount of potassium-40 in the core expressed as a fraction of how much is in the mantle (η_K), the thermal conductivity of the outer core (k_OC), the eruption efficiency (ϵ_erupt), the depression of the viscosity activation energy due to water (﹩{\rm{\Delta }}{E}_{{{\rm{H}}}_{2}{\rm{O}}}﹩), the amount of water the planet formed with (﹩{M}_{p}^{{{\rm{H}}}_{2}{\rm{O}}}﹩), the fraction of that water that is initially in the planet’s atmosphere (﹩{\eta }_{{{\rm{H}}}_{2}{\rm{O}}}﹩), the initial amount of carbon dioxide in the planet’s mantle (﹩{M}_{p}^{{{\rm{CO}}}_{2}}﹩), the reference core liquidus temperature (T_ref,Lind), and the initial average temperature of the mantle (T_m). Each simulation is color-coded based on the identified evolutionary type described in the text. The histograms show the distribution of all simulations marginalized over all variables except for each variable below them.