In this paper we dynamically determine the mass of the Kuiper Belt Objects by exploiting the latest observational determinations of the orbital motions of the inner planets of the Solar System .
Our result , in units of terrestrial masses , is 0.033 \pm 0.115 by modelling the Classical Kuiper Belt Objects as an ecliptic ring of finite thickness .
A two-rings model yields for the Resonant Kuiper Belt Objects a value of 0.018 \pm 0.063 .
Such figures are consistent with recent determinations obtained with ground and space-based optical techniques .
Some implications for precise tests of Einsteinian and post-Einsteinian gravity are briefly discussed .