New and archived high-resolution infrared (IR; 1-20 μm) and radio-continuum images of the isolated embedded cluster and associated compact H II region, GM 24, are presented and measured photometrically. The nucleus of the complex is Irs 3, or IRAS 17136-3617, located at the densest part of the molecular cloud. This object is composed of at least three compact near-IR sources (A, B, and C) that are the most luminous and massive young stellar components and provide most of the ionizing energy to the cometary-shaped radio H II region. The 3.6 cm radio map shows a complex structure with an extended emission peak and two very compact components very close to Irs 3A. Large inhomogeneities in the dust density within the nebula cause considerably different morphologies in the observed emission of hydrogen recombination lines, namely Paβ, Brγ, and Brα. No H2 line emission at 2.12 μm was detected. The embedded IR cluster is found to contain more than 100 members within a radius of around 40'', which corresponds to 0.39 pc. The total stellar mass is estimated to be >=250 M sun. The extinction to the nearby edge of the cluster is determined to be AV = 13, though a number of sources, including Irs 3, are reddened by AV > 50. A fraction of near-IR sources, mainly in the periphery of the cluster, are main-sequence A-B-type stars, while a large fraction (~50%) of the detected members show significant IR excesses, including several Class I young stellar objects with luminosities ranging from a few solar luminosities near our sensitivity limit, to 1.5 × 105 L sun, the derived luminosity of Irs 3.This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile, and with the 2.1 m telescope at the Observatorio Astronómico Nacional at San Pedro Mártir.