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The Carnegie-Chicago Hubble Program (CCHP) is building a direct path to theHubble constant (H0) using Population II stars as the calibrator of the SNIa-based distance scale. This path to calibrate the SN Ia is independent of thesystematics in the traditional Cepheid-based technique. In this paper, wepresent the distance to M101, the host to SN2011fe, using the I-band tip of thered giant branch (TRGB) based on observations from the ACS/WFC instrument onthe Hubble Space Telescope. The CCHP targets the halo of M101 where there islittle to no host-galaxy dust, the red giant branch is isolated from nearly allother stellar populations, and there is virtually no source confusion orcrowding at the magnitude of the tip. Applying the standard procedure for theTRGB method from the other works in the CCHP series, we find aforeground-extinction-corrected M101 distance modulus of{\mu_0}=29.07+/-0.04(stat)+/-0.05(sys) mag, which corresponds to a distance ofD=6.52+/-0.12(stat)+/-0.15(sys) Mpc. This result is consistent with severalrecent Cepheid-based determinations, suggesting agreement between Population Iand II distance scales for this nearby SN Ia-host galaxy. We further analyzefour archival datasets for M101 that have targeted its outer disk to argue thattargeting in the stellar halo provides much more reliable distance measurementsfrom the TRGB method due to the combination of multiple structural componentsand heavily population contamination. Application of the TRGB in complexregions will have sources of uncertainty not accounted for in commonly useduncertainty measurement techniques.

The Carnegie-Chicago Hubble Program. VII. The Distance to M101 via the Optical Tip of the Red Giant Branch Method