  Planetary systems with multiple giant planets provide important opportunities
to study planetary formation and evolution. The HD 45364 system hosts two giant
planets that reside within the Habitable Zone (HZ) of their host star and was
the first system discovered with a 3:2 mean motion resonance (MMR). Several
competing migration theories with different predictions have previously
provided explanations regarding the observed resonance through dynamical
simulations that utilized limited data. Here, over ten years since the original
discovery, we revisit the system with a substantially increased radial velocity
(RV) sample from HARPS and HIRES that significantly extend the observational
baseline. We present the revised orbital solutions for the two planets using
both Keplerian and dynamical models. Our RV models suggest orbits that are more
circular and separated than those previously reported. As a result, predicted
strong planet-planet interactions were not detected. The system dynamics were
reanalyzed, and the planet pair was found to exhibit apsidal behavior of both
libration and circulation, indicating a quasi-resonance state rather than being
truly in MMR. The new orbital solution and dynamical state of the system
confirm migration models that predicted near circular orbits as the preferred
scenario. We also study the habitability prospects of this system and found
that an additional Earth-mass planet and exomoons in the HZ are possible. This
work showcases the importance of continued RV observation and its impact on our
knowledge of the system's dynamical history. HD 45364 continues to be an
interesting target for both planetary formation and habitability studies.
