We perform 3D3V hybrid-Vlasov simulations of turbulence with quasi-isotropic, compressible injection near ion scales to mimic the Earth's magnetosheath plasma, and investigate the novel electron-only reconnection, recently observed by NASA's Magnetospheric Multiscale mission, and its impact on ion heating. Retaining electron inertia in the generalized Ohm's law enables collisionless magnetic reconnection. Spectral analysis shows a shift from kinetic Alfvén waves to inertial kinetic Alfvén and inertial whistler waves near electron scales. To distinguish the roles of inertial scale and gyroradius (d_i and ρ_i), three ion beta (β_i = 0.25, 1, 4) values are studied. Ion-electron decoupling increases with β_i, as ions become less mobile when the injection scale is closer to ρi than di, highlighting the role of ρ_i in achieving an electron magnetohydrodynamic regime at sub-ion scales. This regime promotes electron-only reconnection in turbulence with small-scale injection at β_i ≳ 1. We observe significant ion heating even at large β_i, with Q_i/epsilon ≈ 69%, 91%, and 96% at βi = 0.25, 1, and 4, respectively. While ion heating is anisotropic at β_i≤ 1 (T_i,⊥ > T_i,∥), it is marginally anisotropic at β_i > 1 (Ti,⊥ ≳ Ti,∥). Our results show ion turbulent heating in collisionless plasmas is sensitive to the separation between injection scales (λ_inj and ρ_i, β_i, and finite-k∥ effects, necessitating further investigation for accurate modeling. These findings have implications for other collisionless astrophysical environments, like high-β plasmas in intracluster medium, where processes such as microinstabilities or shocks may inject energy near ion-kinetic scales