  We report on ALMA observations of polarized dust emission at 1.2 mm from
NGC6334I, a source known for its significant flux outbursts. Between five
months, our data show no substantial change in total intensity and a modest 8\%
variation in linear polarization, suggesting a phase of stability or the
conclusion of the outburst. The magnetic field, inferred from this polarized
emission, displays a predominantly radial pattern from North-West to South-East
with intricate disturbances across major cores, hinting at spiral structures.
Energy analysis of CS$(J=5 \rightarrow 4)$ emission yields an outflow energy of
approximately $3.5\times10^{45}$ ergs, aligning with previous interferometric
studies. Utilizing the Davis-Chandrasekhar-Fermi method, we determined magnetic
field strengths ranging from 1 to 11 mG, averaging at 1.9 mG. This average
increases to 4 $\pm 1$ mG when incorporating Zeeman measurements. Comparative
analyses using gravitational, thermal, and kinetic energy maps reveal that
magnetic energy is significantly weaker, possibly explaining the observed field
morphology.
  We also find that the energy in the outflows and the expanding cometary
{\HII} region is also larger than the magnetic energy, suggesting that
protostellar feedback maybe the dominant driver behind the injection of
turbulence in NGC6334I at the scales sampled by our data. The gas in NGC6334I
predominantly exhibits supersonic and trans-Alfvenic conditions, transitioning
towards a super-Alfvenic regime, underscoring a diminished influence of the
magnetic field with increasing gas density. These observations are in agreement
with prior polarization studies at 220 GHz, enriching our understanding of the
dynamic processes in high-mass star-forming regions.
