  tau Ceti is the closest single Sun-like star to the solar system and hosts a
multi-planet system with four confirmed planets. The possible presence of
additional planets, especially potentially habitable worlds, remains of great
interest. We analyze the structure of the tau Ceti planetary system via the
DYNAMITE algorithm, combining information from exoplanet population statistics
and orbital dynamics with measurements of this specific system. We also expand
DYNAMITE to incorporate radial velocity information. Our analysis suggests the
presence of four additional planets, three of which match closely with the
periods of three tentative planet candidates reported previously. We also
predict at least one more planet candidate with an orbital period between
$\sim270-470$ days, in the habitable zone for tau Ceti. Based on the measured
$m \sin i$ values of the confirmed planets, we also assess the possible masses
and nature of the detected and undetected planets. The least massive planets
and candidates are likely to be rocky, while the other planets and candidates
could either be rocky or contain a significant gaseous envelope. The RV
observable signature from the predicted habitable zone planet candidate would
likely be at or just above the noise level in current data, but should be
detectable in future extremely high-precision radial velocity and direct
imaging studies.
