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In gravitational wave (GW) astronomy accurate measurement of the source parameters, such as mass, relies on accurate waveform templates. Currently, the templates are developed assuming that the source, such as a binary black hole (BBH), is residing in a vacuum. However, astrophysical models predict that BBHs could form in gaseous environments, such as common envelops, stellar cores, and accretion disks of active galactic nuclei. Here we revisit the impact of gas on the GW waveforms of stellar-mass BBHs with a focus on the early inspiral phase when the GW frequency is around milli-Hertz. We show that for these BBHs, gas friction could dominate the dynamical evolution and hence duplicate chirp signals. The relevant hydrodynamical timescale, $τ_{\rm gas}$, could be much shorter than the GW radiation timescale, $τ_{\rm gw}$, in the above astrophysical scenarios. As a result, the observable chirp mass is higher than the real one by a factor of $(1+τ_{\rm gw}/τ_{\rm gas})^{3/5}$ if the gas effect is ignored in the data analysis. Such an error also results in an overestimation of the source distance by a factor of $(1+τ_{\rm gw}/τ_{\rm gas})$. By performing matched-filtering analysis in the milli-Hertz band, we prove that the gas-dominated signals are practically indistinguishable from the chirp signals of those more massive BBHs residing in a vacuum environment. Such fake massive objects in the milli-Hertz band, if not appropriately accounted for in the future, may alter our understanding of the formation, evolution, and detection of BBHs.