  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 +/- 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 +/- 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.
