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The observed correlation between outer giant planets and inner super-Earthsis emerging as an important constraint on planet formation theories. In thisstudy we focus on Kepler-167, which is currently the only system known tocontain both inner transiting super-Earths and a confirmed outer transiting gasgiant companion beyond 1 au. Using long term radial velocity monitoring, wemeasure the mass of the gas giant Kepler-167e ($P=1071$ days) to be$1.01^{+0.16}_{-0.15}$ M$_{\rm J}$, thus confirming it as a Jupiter analog. Were-fit the $Kepler$ photometry to obtain updated radii for all four planets.Using a planetary structure model, we estimate that Kepler-167e contains$66\pm19$ M$_{\oplus}$ of solids and is significantly enriched in metalsrelative to its solar-metallicity host star. We use these new constraints toexplore the broader question of how systems like Kepler-167 form in the pebbleaccretion framework for giant planet core formation. We utilize simple diskevolution models to demonstrate that more massive and metal-rich disks, whichare the most favorable sites for giant planet formation, can also deliverenough solids to the inner disk to form systems of super-Earths. We use thesesame models to constrain the nature of Kepler-167's protoplanetary disk, andfind that it likely contained $\gtrsim 300$ M$_{\oplus}$ of dust and was$\gtrsim 40$ au in size. These values overlap with the upper end of theobserved dust mass and size distributions of Class 0 and I disks, and are alsoconsistent with the observed occurrence rate of Jupiter analogs around sun-likestars.

Kepler-167e as a Probe of the Formation Histories of Cold Giants with Inner Super-Earths