The bulk of the quiet solar photosphere is thought to be significantly magnetized, due to the ubiquitous presence of a tangled magnetic field at subresolution scales with an average strength langBrang ~ 100 G. This conclusion was reached through detailed three-dimensional (3D) radiative transfer modeling of the Hanle effect in the Sr I 4607 Å line, using the microturbulent field approximation and assuming that the shape of the probability density function of the magnetic field strength is exponential. Here, we relax both approximations by modeling the observed scattering polarization in terms of the Hanle effect produced by the magnetic field of a 3D photospheric model resulting from a (state-of-the-art) magneto-convection simulation with surface dynamo action. We show that the scattering polarization amplitudes observed in the Sr I 4607 Å line can be explained only after enhancing the magnetic strength of the photospheric model by a sizable scaling factor, F ≈ 10, which implies langBrang ≈ 130 G in the upper photosphere. We also argue that in order to explain both the Hanle depolarization of the Sr I 4607 Å line and the Zeeman signals observed in Fe I lines, we need to introduce a height-dependent scaling factor, such that the ensuing langBrang ≈ 160 G in the low photosphere and langBrang ≈ 130 G in the upper photosphere.