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Line-intensity mapping (LIM) experiments coming online now will surveyfluctuations in aggregate emission in the [C II] ionized carbon line fromgalaxies at the end of reionization. Experimental progress must be matched bytheoretical reassessments of approaches to modelling and the informationcontent of the signal. We present a new model for the halo-[C II] connection,building upon results from the FIRE simulations suggesting that gas mass andmetallicity most directly determine [C II] luminosity. Applying our new modelto an ensemble of peak-patch halo lightcones, we generate new predictions forthe [C II] LIM signal at $z\gtrsim6$. We expect a baseline 4000-hour LIM surveyfrom the CCAT facility to have the fundamental sensitivity to detect the [C II]power spectrum at a significance of $4\sigma$ at $z\sim6$, with an extended orsuccessor Stage 2 experiment improving significance to $36\sigma$ at $z\sim6$and achieving $8\sigma$ at $z\sim7.5$. Cross-correlation through stacking,simulated against a mock narrow-band Lyman-break galaxy survey, would yield astrong detection of the radial profile of cosmological [C II] emissionsurrounding star-forming galaxies. We also analyse the role of a few of ourmodel's parameters through the pointwise relative entropy (PRE) of thedistribution of [C II] intensities. While the PRE signature of different modelparameters can become degenerate or diminished after factoring in observationaldistortions, various parameters do imprint themselves differently on theone-point statistics of the intrinsic signal. Further work can pave the way toaccess this information and distinguish different sources of non-Gaussianity inthe [C II] LIM observation.

The informativeness of [C II] line-intensity mapping as a probe of the H I content and metallicity of galaxies at the end of reionization